From the result of fitting to the nuclear data, one can guess that true \(K_0\)  value may be located in \(K_0 = 230-250\)  MeV.
However, it is premature to draw a definite conclusion because
density of nuclei is identically close to \(\rho _0\) , so the information about the density dependence of the EoS
one can obtain from the nuclear data might be limited.
In addition, asymmetry \(\delta \)  of \(^{48}\) Ca and \(^{208}\) Pb are 0.17 and 0.21, respectively,
so they are not large enough to magnify the effect of the symmetry energy.
Neutron stars provide environment with more wider density range and the large neutron-proton asymmetry.
Not abandoning the possibility of small or large \(K_0\)  value, we include \(K_0=220\)  and 260 MeV in the consideration of the neutron star.
For each \(K_0\)  value, (\(J\) , \(L\) , \(K_\tau \) ) values are chosen from the two smallest \(\chi _6^2\)  values.
Equation of state parameters thus determined are summarized in Tab. REF .
Ranges of \(J\)  and \(L\)  in Tab. REF  are \(30-34\)  MeV and \(40-70\)  MeV, respectively.
These ranges are similar to the experimental ranges adopted in [1]}.
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